In Fig. 5 we show our results
for \(\Lambda \)  as a function of the star mass \(M\) .
As it can be seen, the constraint (REF ) can be satisfied.
We note, however, the visible tension between this constraint and those
shown in the mass-radius plot. The larger values of the radius required
to fit the NICER points seem to be somewhat difficult to reconcile with the
\(\Lambda \)  values required by the GW170817 estimates. Other calculations
performed with quark matter stars [1]}, [2]}, [3]}, [4]}, [5]} or hybrid
stars [6]}, [7]}, [8]}, [9]}, [10]}, [11]} arrive at similar results.
On the other hand,
calculations of the tidal deformability with purely hadronic equations of
states [12]}, [13]}, [14]} seem to reproduce the experimental data
more easily.
<FIGURE>